Mercury surface temperature
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Mercury Surface Temperature: Variations and Influences
Extreme Temperature Variations on Mercury
Mercury experiences some of the most extreme temperature variations in the solar system. Due to its proximity to the Sun and its slow rotation, the surface temperatures on Mercury can vary dramatically between day and night. At the equator, temperatures can soar up to 700 K (427°C) at local noon and plummet to less than 100 K (-173°C) during the night1. This significant fluctuation is primarily due to the planet's 3:2 spin-orbit resonance, which causes certain longitudes to experience local noon at perihelion, resulting in "hot" poles, while others experience it at aphelion, resulting in "warm" poles1.
Observations and Measurements
Historical Observations
Early observations of Mercury's temperature were conducted using radio emissions. Measurements from the University of Michigan in the 1960s suggested that the sub-solar point on Mercury could reach temperatures as high as 1100 K, although this was based on the assumption that the dark side of Mercury had a temperature close to zero2. These early estimates highlighted the need for more precise measurements and models.
Mariner 10 and MESSENGER Missions
The Mariner 10 mission provided infrared brightness temperature data, revealing that the minimum predawn surface temperature at the warm pole (longitude 270°) was around 93 K3. The MESSENGER spacecraft further refined our understanding by providing detailed surface composition and temperature data, which have been used to develop thermal models of Mercury's regolith5.
Thermal Models and Regolith Properties
Thermal models of Mercury's surface and subsurface have been developed to understand the impact of physical heterogeneities on surface temperature. These models consider factors such as thermal conductivity, heat capacity, and porosity, which can cause significant variations in temperature, especially during twilight and nighttime5. The regolith's thermal inertia, which is similar to that of the Moon, plays a crucial role in these temperature variations4.
Polar Regions and Water Ice Stability
Despite Mercury's high daytime temperatures, its polar regions can harbor water ice. Radar observations have detected high radar reflectivity near Mercury's poles, which is consistent with the presence of water ice. Thermal models indicate that temperatures in permanently shadowed craters at the poles can be as low as 60 K, allowing water ice to remain stable over geological timescales8.
Conclusion
Mercury's surface temperature is characterized by extreme variations due to its unique orbital and rotational dynamics. Observations from missions like Mariner 10 and MESSENGER, along with advanced thermal models, have provided a detailed understanding of these temperature fluctuations and their implications for the planet's surface and subsurface properties. The presence of water ice in the polar regions further adds to the complexity of Mercury's thermal environment, highlighting the diverse and dynamic nature of this innermost planet.
Sources and full results
Most relevant research papers on this topic
Estimation of surface temperatures on Mercury in preparation of the MERTIS experiment onboard BepiColombo
The surface of Mercury experiences large temperature variations, with temperatures reaching up to 700 K at local noon at the equator and 570 K at longitudes 90° W and 270° W, depending on solar irradiation.
Mariner 10 infrared radiometer results - Temperatures and thermal properties of the surface of Mercury
Mariner 10 infrared data reveals that Mercury's surface temperatures are similar to those found on the Moon, with thermal inhomogeneities and electrical properties similar to those found on the Moon.
Mercury: The Dark-Side Temperature
The average dark-side temperature of Mercury is 111 3 K, suggesting similar top surface layers to the moon.
Thermal model of Mercury’s surface and subsurface: Impact of subsurface physical heterogeneities on the surface temperature
Subsurface physical heterogeneities significantly impact Mercury's surface temperature, particularly at twilight and during the night, and may even affect the absolute level of surface temperature due to topography and textural properties.
Temperature dependence of the surface energy of mercury from 0 to 250°C
The surface energy of mercury is temperature-dependent, with ideal agreement achieved between calculated and experimental data for temperatures 0 to 250°C.
The Effect of Temperature on the Structure of Mercury
Mercury's structure changes with temperature, revealing a new peak and a small subsidiary peak that changes position more rapidly than the others.
The Thermal Stability of Water Ice at the Poles of Mercury
Water ice may exist at Mercury's poles, where temperatures are expected to be below 112 kelvin, making it stable to evaporation over billions of years.
Highly CitedMelting processes and mantle sources of lavas on Mercury
Mercury's surface basalts were produced by partial melting of enriched lherzolitic mantle sources, supporting strong secular cooling of the mantle between 4.2 and 3.7 Ga.
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